It is therefore important to use independent methods
to verify ine distances to globular clusters, especially methods which are not effected by the reddening of stars. In this paper we use data from the Gaia EDR3 catalogue [1]}, [2]}
to determine distances to Galactic globular clusters. In addition to using the Gaia EDR3 parallaxes directly, we also determine moving group distances and kinematic distances derived by comparing proper motion velocity dispersion
profiles with line-of-sight velocity dispersion ones. We finally use the Gaia EDR3 parallaxes of nearby subdwarfs as well as
Hubble Space Telescope (HST) star counts together with kinematic information to determine distances.
